Our results show that GW170729 is the largest mass binary black hole signal and GW170608 is the smallest mass binary black hole signal from the detections during O1 and O2. Parameter estimates of the binary black holes observed during O1 were presented in Refs. [1]}, [2]}.
GW170814 seems to have lesser support for asymmetric mass ratios than the other events. All the events have low effective spin values. GW170814 has more support for face-on systems, whereas GW170809 and GW170818 has a preference for face-off systems. For GW170608, there is preference for both face-on (\(\iota = 0\) ) and face-off (\(\iota = 180\) ). GW170104, GW170729, and GW170823 has support for face-on (\(\iota = 0\) ), face-off (\(\iota = 180\) ) and edge-on (\(\iota = 90\) ). Face-on systems are those for which the inclination angle \(\iota = 0\) ; ie. the line of sight is parallel to the binary's orbital angular momentum. Face-off systems are those for which \(\iota = \pi \)  (the line of sight is anti-parallel to the binary's orbital angular momentum). We also computed \(\chi _{p}\)  for each of the events and found no significant measurements of precession. GW170608 seems to be observed at the closest luminosity distance and GW170729 the farthest among the O2 binary black holes.
